Institute for Cosmic Ray Research University of …cosmic ray in the Galaxy and the heliosphere On...
Transcript of Institute for Cosmic Ray Research University of …cosmic ray in the Galaxy and the heliosphere On...
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Precision research of cosmic rays
from space after 10 years of
PAMELA observations
M. Casolino
RIKEN
INFN
University of Rome Tor Vergata
19/03/2017
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M. Casolino, INFN & University
Roma Tor Vergata
… 1989 1990 1991 1992 1993 1994 1995 1996 1997 1998 1999 2000 2001 2002 2 2006- 2017
Past, present and future experiments
C 94 C 97 C 98 TS 93 M 89 M 91
MASS-89, 91, TS-93,
CAPRICE 94-97-98
PAMELA
PAMELA
NINA-2
NINA-1
NINA-1 NINA-2
SILEYE-2 SILEYE-
1
SILEYE-3/
ALTEINO:
SILEYE-
4/ALTEA
SILEYE-1 SILEYE-2 SILEYE-3 ALTEA
LAZIO-SIRAD
LAZIO-SIRAD
JEM-EUSO
CSES
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Pamela Collaboration
Moscow
St. Petersburg
Russia:
Sweden:
KTH, Stockholm
Germany: Siegen
Italy:
Bari Florence Frascati Trieste Naples Rome CNR, Florence
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M. Casolino - INFN & University of Roma Tor Vergata\
Integration in Baikonur cosmodrome,
Spring 2006
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Pamela during integration in Baikonur Resurs DK integrated
Coupling to Soyuz
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M. Casolino - INFN &
University of Roma
Tor Vergata\
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Gagarinsky Start, 14/6/2006
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Launch on June 15th 2006 Soyuz-U rocket
70 degrees polar orbit
350*600km elliptical
600km circular
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Magnetic (0.46T)
Spectrometer
Microstrip
detector (6 double sided
microstrip planes)
Silicon
Tungsten
Tracking
Calorimeter (44 planes of 96 strip)
Shower
Catcher
Scintillator
Neutron
Detector
Time
of Flight (three scintillators,
6 planes, 48 phototubes)
The detector
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Electrons Positrons Protons
Principle of detection
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ApJ 457, L 103 1996
ApJ 532, 653, 2000
arXiv:0810.4994, PRL,
NJP11,105023
Nature,
Astrop. Phys
Science 2011
arXiv:1103.4055
ApjL 799 4 2015
2008AdSpR..41..168C
2008AdSpR..41.2037D
2008AdSpR..41.2043C
Prl 111 1102 203
PrL 106 1101 2011
PrL105 121101 2010 --
High precision cosmic ray measurements challenge and constrain models of production, acceleration and propagation of cosmic ray in the Galaxy and the heliosphere On several different scales Modeling
Dose and risk
estimation for astronauts on ISS and Moon/Mars
Physics Reports
544, 4, 323-370, 2014 Apj 795 91 2013
Apj 770 2 2013
Apj 791 2 2014
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Charged cosmic ray spectrum
•Power law spectrum
•Solar Modulation
•Galactic Cosmic Rays
•Extragalactic Cosmic
Rays
Adapted from Simpson 1983 in PDG by M. Casolino
LHC
JEM-EUSO K-EUSO
PAMELA Altea
Alteino
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Direct e+ / e- P / P-
Pamela Physics objectives and the Hillas Plot
Jem-Euso
K-Euso
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1) Direct violation of baryonic number
particle “X” decays breaking baryon symmetry 2) CP violation
to avoid specular antiparticle decay
3) Non thermal equilibrium at a given time
To avoid baryon compensation through inverse processes
Sakharov, A.D. 1967, J. of Exper. and Theo. Phys. Letters, 5, 24-28, “Violation of CP Invariance, C Asymmetry, and Baryon Asymmetry of the Universe”
(Russian: Андре́й Дми́триевич Са́харов) (May 21, 1921 – December 14, 1989)
Sakharov conditions
Matter / Antimatter Asymmetry in the Universe
Cosmological scale (beyond Cosmic Microwave Background)
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PAMELA (2006-2009)
JEPT letters 93, 11,
628-631, 2011
Search for antinuclei
Antihelium also
from primordial
nucleosyinthesis
Antinuclei only
from antistars
Pamela (2006-2009)
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Search for exotic matter: Strangelets (Lumps of Strange Quark Matter)
u,d,s quark matter
might be stable
Not limited in A
A=100, 1000….
Z is almost zero due to
cancellation of quark
charge
Could account for a
(small) part of DM
Also candidate of
UHECR
Roughly equal numbers of u,d,s quarks in a
single ‘bag’ of cold hadronic matter.
7 Z=2 A=4 (He)
Z/A=0.5 Z=2 A=7
Z/A=0.286
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Strangelet upper limit
PRL 115, 111101 –
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Cosmic rays on Galactic scale:
Nuclei, protons, antiprotons, isotopes
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Cosmic rays are accelerated in Supernova explosions
(probably) • Meet energy criteria
• First order Fermi shock acceleration produces power law spectrum
• Observed in gamma by Agile and Fermi
Keplers’ supernova
Tycho’s supernova
– HESS TeV emision from SNR RX J1713.7-3946 hadronic inter. Of cr. E>10^14eV F. Aharonian, et al., Astron. Astrophys. 464, 235 (2007).
– X-ray measurements of the same SNR evidence that protons and nuclei can be accelerated E>10^15 eV in young SNR Uchiyama, et al., Nature 449, 576 (2007).
– AGILE: diffuse gamma-ray (100 MeV – 1 GeV) SNR IC 443 outer shock hadronic acceleration M. Tavani, et al., ApJL 710, L151 (2010).
– Fermi: Shell of SNR W44 have decay of pi0 produced in the interaction of hadrons accelerated in the shock region with the interstellar medium A. Abdo, et al., Science 327, 1103 (2010).
– Starburst galaxies (SG), where the SN rate in the galactic center is much higher than in our own, the density of cosmic rays in TeV gamma-rays (H.E.S.S infers cosmic rays density in SG NGC 253 three orders of magnitude higher than in our galaxy F. Acero, et al., Science 326, 1080 (2009).
– VERITAS: SG M82 cosmic rays density is reported to be 500 times higher than in the Milky Way VERITAS Collaboration, et al., Nature 462, 770 (2009
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Pamela galactic proton and He
2006-2008
30- 1000GV, p = 2.820 +- 0.003 (stat) +- 0.005 (syst)
30- 1000GV, he = 2.732 +- 0.005 (stat)
+ 0.008 -0.003 (syst)
• Different spectral index
for proton and helium.
• Helium percentage is
growing with rigidity
• Challenges Supernova
only origin of cosmic
ray and/or
acceleration/propagation
models.
Science 2011, 332 no. 6025 pp. 69-72
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Global picture: PAMELA & AMS-02 proton spectrum
Solar modulation
O. Adriani et al, Phys. Rep. (2014)
0.988
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Global picture: PAMELA & AMS-02 helium nuclei spectrum
Solar modulation
1.036
O. Adriani et al, Phys. Rep. (2014)
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-0.101+-0.002
Ratio P/He: Rigidity
Solar modulation 230-240GV
1. Acceleration is
a rigidity
dependent
effect
2. The ratio
decreases
More He at
high energies
Acceleration
mechanisms or
sources are
different?
3. Measurement
valid also
below the (low)
solar
modulation
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Acceleration / Propagation is a
rigidity phenomenon
Total Kinetic energy
Kinetic energy/ nucleon
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At higher energies: Cream and ATIC data
Ahn et al, ApJL 2010
200 GeV/n (PAMELA at 120 GeV/n)
Indirect p, He Direct C-Fe
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Conclusion from Proton and Helium
Proton and Helium undergo different processes
even in GeV-TeV scale
Change in spectral index around 230-240GV
Needed to bridge to high energy
Various hypotesis to explain Pamela data
Additional Sources Wolfendale 2011, 2012
Spallation, Propagation Blasi & Amato 2011, 2013
Weak local component (+ others) Vladimirov,
Johanesson, Moskalenko 2011
Reacceleration Thoudam & Horandel, 2013
Various models, Moskalenko 1108.1023
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B/C ratio Propagation in the Galaxy
• B/C ratio
Secondary/primay
CNO+ISM B
Propagation in the
Galaxy
Time of permanence of cr
ApJ 791 2 2014
BCNOescCB σλN/N
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Puzzle of production and
propagation in the galaxy
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H and He Isotopes Propagation in the Galaxy
• Flux depends on
solar modulation
• Ratio is less
dependent
• Strong tool for
evaluating
secondary particle
production in the
galaxy
• Complementary to
B/C
ApJ 770:2, 2013
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Antiprotons
• Secondary production, kinematics well
understood
• Probe for extra sources
• Galactic scale
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Discovery of antiprotons in cr, 1979
• p/p ratio
6 x 10-4
• 2-5 GeV
Bogomolov, E.A. et al. 1979, Proc. 16th ICRC, Kyoto, 1, 330, “A Stratospheric Magnetic Spectrometer Investigation of the Singly Charged Component
Spectra and Composition of the Primary and Secondary Cosmic Radiation”
From
Robert E. Streitmatter
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Robert L. Golden
Also Golden, 1979
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Indirect Dark matter search in space
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Antiproton/proton ratio
Low Energy
Confirms charge
dependent solar
modulation
High Energy
Consistent with
models (Galprop,
Donato…)
PRL. 105, 121101, 2010
PRL 102:051101,2009
Simon et al. (ApJ 499 (1998) 250) Ptuskin et al.
ApJ 642 2006 902
Donato et al. (PRL 102 (2009) 071301)
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Antiproton absolute flux
Apparently no
extra sources
Rule out and
strongly
constrain many
models of DM
S M. Asano, et al, Phys. Lett. B 709 (2012) 128.
R. Kappl et al , PRD 85 (2012) 123522
M. Garnyet al, JCAP 1204 (2012) 033
D. G. Cerdeno, et al, Nucl. Phys. B 854 (2012) 738
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Galactic neighborhood:
e+, e- (1-2 kpc)
Synchrotron Radiation and
Inverse Compton
Limit propagation to 1-2 kpc
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M. Casolino, INFN & University
Roma Tor Vergata
Nature 458, 607-609 ( 2009)
Charge
dependent solar
modulation
increase over background
Pamela positron fraction
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M. Casolino, INFN & University
Roma Tor Vergata
Pamela positron fraction:
comparison with other data
Nature 458, 607-609 (2 April 2009)
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AMS & FERMI have confirmed PAMELA data
Charge
dependent solar
modulation L. Maccione, PRL
110 (2013) 081101
Anomalous
source at high
energy
Charge dependet
Solar modulation
at low energy
Need 3D
model of
heliosphere
.
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Absolute positron spectrum
PRL 111 2013
Propagation
Charge
dependent solar
modulation
PRL111, 081102 (2013)
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M. Casolino, INFN & University
Roma Tor Vergata
Secondary production
Dark Matter Annihilation
Astrophysical sources, SNR…
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Heliosphere and long term solar modulation
(100 AU)
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M. Casolino, INFN & University
Roma Tor Vergata
Solar modulation at minimum of solar cycle 23-24: 2006-2013
BESS
Caprice / Mass /TS93
AMS-01
Pamela
A+ A+ A- A- A-
Note different shape of proton
Charge dependent solar modulation
A+
PAMELA
Wizard-Balloon
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Solar modulation of protons and nuclei: monthly
ApJ 765, 2, 91, (2013)
Very long and peculiar
solar minimum.
Current solar cycle (24)
late and weak.
Closer to interstellar
medium.
Good reference field
for dosimetry
interstellar flux
From V. Formato
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Very long and peculiar
solar minimum.
Current solar cycle (24)
late and weak.
Closer to interstellar
medium.
Good reference field
for dosimetry
interstellar flux
ApJ 765, 2, 91, (2013)
Solar modulation of protons and nuclei: monthly
2010 Decreasing
Solar activity
Increasing
Galactic flux
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•Charge dependent solar modulation
•Separate qA>0 with qA<0 solar cycles
•Evident in the proton flux
•Observed in the antiproton channel by
BESS
•Full 3D solution of the Parker equation
– drift term depends on sign of the
charge
Charge dependent solar modulation of low energy positrons
BESS
Caprice / Mass /TS93 AMS-01
Pamela
Miyake, Yanagita, 2008
A+ A-
A<0 (2010) p,e+
A<0 (2010) p-,e-
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Charge dependent solar modulation: PAMELA electron and positron spectra over the last solar minimum
Variation of the e-, e+ and p flux between Jul 2006 and December 2009
Norm
aliz
ed f
lux
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Solar particle events (1 AU)
Dec 13th largest CME since 2003, anomalous at sol min
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December 13th 2006 event
ApJ 742, 2, 102, 11, 2011.
No simple modeling
of acceleration and
propagation
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PAMELA SEP Spectra
100 MeV 1 GeV Proton Energy
Flux
Completing the spectrum PAMELA bridges the gap between low energy space-based and ground-‐based measurements to obtain a complete spectrum
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M. Casolino, INFN & University
Roma Tor Vergata
Forbush decrease
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M. Casolino, INFN & University
Roma Tor Vergata From Mergè Martucci Sotgiu
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GEOMAGNETOSPHERE, VAN ALLEN BELTS
PAMELA
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Selection of galactic component according to
geomagnetic cutoff
Rcutoff=14.9GV/L2
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M. Casolino, INFN & University
Roma Tor Vergata
Pamela maps at various altitudes
http://www.youtube.com/watch?v=OaoiPw5Pqbg
Geomagnetosphere, Van Allen Belts
(1000 km)
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RED: JULY 2006
BLUE: AUGUST 2007
P/(
cm^2
sr
GeV
s)
Galactic protons
Primary (galactic) spectra:
polar measurements
M. Honda, 2008
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RED: JULY 2006
BLUE: AUGUST 2007
P/(
cm^2
sr
GeV
s)
Primary and secondary spectra:
Intermediate latitudes
Secondary particles (reentrant albedo)
Penumbra
M. Honda, 2008
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RED: JULY 2006
BLUE: AUGUST 2007
P/(
cm^2
sr
GeV
s)
Secondary particles
Penumbra M. Honda, 2008
Primary and secondary spectra:
Magnetic equator
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JULY 2006 AUGUST 2007
Proton Flux at various cutoff
P/(
cm^2 s
r G
eV s
)
Subcutoff
(secondary albedo)
Particles
•P, e-,e+, P-
•Grigorov, Sov. Phys.
Dokl. 22, 305 1977
•NINA results:
•ApJ Supp.132 365,
2001
•AMS results:
Phys. Lett. B 472
2000.215,
Phys. Lett. B 484
2000.10–22
•G. Esposito PhD
•+calculations
•Lipari, Astrop. Ph. 14,
171, 2000
•Huang et al, Pys Rev. D
68, 053008 2003
•Sanuki et al, Phys Rev
D75 043005 2007
•Honda et al, Phys Rev
D75 043006 2007
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Integral fluxes at different GC altitudes, averaged over the explored pitch angle range
arXiv:1412.1765 , ASR 2016
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Integral fluxes at different GC altitudes, averaged over the explored pitch angle range
arXiv:1412.1765 , ASR 2016
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Integral fluxes at different GC altitudes, averaged over the explored pitch angle range
arXiv:1412.1765 , ASR 2016
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Integral fluxes at different GC altitudes, averaged over the explored pitch angle range
arXiv:1412.1765 , ASR 2016
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Integral fluxes at different GC altitudes, averaged over the explored pitch angle range
arXiv:1412.1765 , ASR 2016
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O. Adriani et al. 2011 ApJ 737 L29
Discovery of stably trapped antiprotons in Earth’s radiation belt
Total mass
Less than ng
Negligible but
replenishable
Saturn, Jupiter
mass mg
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M. Casolino, INFN & University
Roma Tor Vergata
•Expected three years of operations – survived 10!
•Data analysis is in progress
•Data available on ASI science data center (ASDC)
http://pamela.roma2.infn.it
http://www.casolino.it
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1. EUSO-TA: Ground
detector installed in 2013 at
Telescope Array site:
currently operational
2. EUSO-BALLOON: 1st
balloon flight from Timmins,
CA (French Space Agency)
Aug 2014; NASA Ultra long
duration flight: 2017
3. MINI-EUSO (2017): Precursor from International
Space Station (ISS: 30kg
2017). Approved by Italian
and Russian Space agencies
4. K-EUSO (2022): ISS
Approved by Russian Space
Agency
The EUSO program Ultra-High Energy
cosmic rays from space
MINI-EUSO
(2017)
400 km
EUSO-TA (2013-)
EUSO-TA (2013)
EUSO-BALLOON (2014)
EUSO-SPB (2017)
40 km
(2022) JEM-EUSO
(2023+)